1) Hogerheijde's counter-rotating disks:
"   I might have a neat picture for the CARMA booth, with recent results on
HCO+ 1-0 and 3-2 emission from a contracting, rotating disk around a young
star. It contains data from BIMA (HCO+ 1-0 and 3-2) and OVRO (1-0); the
HCO 1-0 image contains data from both arrays ("virtual" CARMA)."
 

2) Rick Forester's M87 and Carma Move pictures:

a) M87 polarization map at 3 mm.

b) Planned move of the BIMA antennas (joke!)

3) Fabian Walter's contribution:

"dwarfs are a good example why we need more powerful radio interferometers
such as carma.  the reasoning would be that dwarf galaxies are important
targets to study since they are believed
to be the nearby counterparts of the young galaxy population at large
redshift (metal poor, small, blue, actively forming stars). the fact that
they are small and metal poor makes it so far very difficult to study
their molecular gas phase which is vital to understand star formation in
these systems. only the next generation of mm interferometers such as
carma will allow us to study the properties of the interstellar medium in
these objects in much greater detail."

4) M51 montage from Stuart Vogel:  A rosetta stone galaxy:

M51 from OVRO - Scoville / Poletta

5)  My contributions: - BIMA SONG Gallery:
" CARMA will allow us to get an instant photograph of the molecular gas in nearby and distant galaxies.  Today, with the
existing arrays such studies push the limits of technology - the 44 galaxies BIMA survey took over a year and a half.  And the OVRo survey which imaged a smaller region in 20 galaxies also took a significant amount of time.  CARMA will not only
do this faster, with higher sensitivity but it will also allow for imaging of larger areas of the galaxies.  We will be able
to study the morphology and kinematics of the molecular gas, the fundamental fuel for star formation and galaxy evolution."

6) Tony's initial science pages:

8) Dick Plambeck's contribution:

9) Micol Christopher's Galactic Center Data

The center of our Milky Way Galaxy contains a black hole with a mass of
several million suns.  This massive black hole, which lies only 20,000
light years from earth, provides astronomers with a unique opportunity to
study the environements around massive black holes, which is made
particularly interesting because many galaxies are thought to contain such
black holes in their centers.  Using OVRO, we mapped molecular gas (HCN)
and ionized gas (appearing as continuum emission) within the inner 10
light years of our galaxy.  The HCN distribution is shown by the color
image and the continuum emission by contours.  HCN particularly emphasizes
regions of high density. From the image one can see clearly a ring-like
structure of molecular gas surrounding the galactic center; this has
become known as the Circumnuclear Disk.  Also interesting is the interplay
between the ionized and molecular gas - along the western part of the
ring, the ionized gas appears to mark the inner boundary to the ring,
while to the north the ionized gas seems to be "escaping" through an area
of lower molecular gas concentration in the ring.  With OVRO, we are also
able to measure the radial velocities of the HCN, and with this
information we hope to model the action of the molecular gas, both in its
likely orbit around the galactic center but also in its possible infall
onto the black hole.
 

10) Shardha's NGC 2782 contribution

"Theory and simulations suggest that a nuclear stellar bar provides an
efficient way of fueling  gas into a central starburst or AGN.
OVRO  CO (1-0) observations  of NGC 2782 reveal one of the first cases
where  a nuclear stellar bar is caught  feeding molecular gas into a
central starburst.  The CO map   (contours) at 1.5'' resolution  overlaid
on the 5 GHz radio continuum (greyscale), shows  a clumpy bar-like molecular
feature of mass $2.5 \times 10^9$ $\msun$ with weak bar-like streaming motions.
The gas lies  on the leading side of a  nuclear stellar bar where gravitational
torques  will cause it to lose angular momentum and fuel the central starburst
which is driving a dynamically  young outflow."
 

To elucidate the origins of high nuclear star formation rates, a comparative
study of the molecular gas in the brightest nearby starbursts comparable to M82,
and control non-starbursts has been conducted.  The figure shows the CO
intensity  (contours) of typical resolution  2'' (100--200 pc)  on the star formation
(greyscale).  In the starbursts which have  a high SFR  per unit mass of
molecular gas, the peak  gas  density is high (1000 to  3500 $\msun$ pc$^{-2}$), and the
local  gas  density is close to the Toomre critical density for the onset of
gravitational instabilities.  Conversely, in  the non-starbursts, sub-critical densities
and  large local velocity gradients or shear appear to inhibit star formation
in several gas-rich regions.
 

11) Geoff + Gurwell...

12) HH212 from Chin Fei Lee, left (h2), middle is CO and right one is an overlay.  Blue star is the ionizing star.

13) Hot cores from Friedrich Wyrowski

"Hot Core figure: Subarcsecond resolution BIMA observations of the
     1.3mm dust continuum toward hot core/ultracompact HII regions
     resolve sites of massive (proto) stars before (G9/G29) or
     shortly after (G10) the formation of ultracompact HII regions
     as seen by the 1.3cm free-free emission (Cesaroni et al. 1994/1998).
     Close to the dust cores detected with BIMA, other more evolved
     UCHIIs have already dispersed their parential gas and dust
     reservoir. The spectrum in the lower left panel shows many lines
     of highly excited complex molecules as typical characteristics
     of the hot molecular gas surrounding massive (proto) stars."

And..
"IRDC figure:   High-angular-resolution BIMA observations of N2H+ (1-0)
     reveal cold and dense condensations within a new population of
     infrared-dark clouds identified during the MSX mid-infrared
     survey of the Galactic Plane (Egan et al. 1998). "

14) Lots of HH objects fron CF Lee's thesis - made by Vogel